Angular resolution of the LISA gravitational wave detector

摘要: We calculate the angular resolution of planned LISA detector, a space-based laser interferometer for measuring low-frequency gravitational waves from galactic and extragalactic sources. is not pointed instrument; it an all-sky monitor with quadrupolar beam pattern. will measure simultaneously both polarization components incoming waves, so data consist two time series. All physical properties source, including its position, must be extracted these LISA's therefore fixed quantity, but rather depends on type signal how much other information extracted. Information about source position encoded in measured three ways: (1) through relative amplitudes phases components, (2) periodic Doppler shift imposed by detector's motion around Sun, (3) further modulation caused time-varying orientation. derive basic formulas required to $\ensuremath{\Delta}{\ensuremath{\Omega}}_{S}$ given source. then evaluate sources particular interest: monchromatic mergers supermassive black holes. For types sources, we (in high signal-to-noise approximation) full variance-covariance matrix, which gives accuracy all parameters can measured. Since our results depend mainly gross features detector geometry, orbit, noise curve, expect fairly insensitive modest changes design that may occur between now launch. also calculations could easily modified apply design.